The superaccretor SS 433 belongs to a typical class of ULXs. The apparent X-ray luminosity is about \(\sim 10^{36}\)  erg s\(^{-1}\)  but the intrinsic luminosity is considered to be probably
\(\ge 10^{39}\)  erg \(s^{-1}\)  because we observe the source edge-on (Fabrika 2004, Fabrika, Vinokurov and Atapin 2018).
In our models Thick4 and 5, the luminosities are very high as \(\sim 10^{40}\)  erg s\(^{-1}\)  and
the radiation shows a strongly anisotropic distribution around the rotational axis.
In addition, the edge-on luminosity through the outer radial boundary is very low as \(\sim 10^{36}\)  erg s\(^{-1}\) .
The large mass outflow rates \(\dot{M}_{\rm out} \sim 10^{-5}\)  – \(10^{-4} M_{\odot }\) 
yr\(^{-1}\)  are originated in the wide wind region. However, the relativistically high velocity jets
along the rotational axis are not found in the funnel region, as is detected in SS 433. This may be due to that the outer boundary used here is small as \(R_{\rm out}\)  = 100
and the outflow gas in the funnel region is not still sufficiently accelerated by powerful radiation
pressure force.
In SS 433 which consists of a close binary system,
the mass transfer rate from the second companion and the wind mass outflow rate from the primary
are observationally estimated to be \(\sim 10^{-4}\)  – \(10^{-3} M_{\odot }\)  yr\(^{-1}\) 
and \(\sim 10^{-5}\)  – \(10^{-4} M_{\odot }\)  yr\(^{-1}\) , respectively [1]}.
Their values agree well to the input mass
accretion rates and the mass outflow rates in models Thick4 and 5.
In the close binary system with high luminosity, it is conceivable that the companion
transports not only high mass outflow but also high angular momentum to the primary through critical
Roche lobe, differently from small angular momentum by stellar wind in detached binary system.
Then, one may wonder if the inviscid flow used in this paper is valid under such close binary system with the super-Eddington luminosity or not.
This is justified as the viscous flow can achieve specific angular momentum of Keplerian value at the outer boundary while behaving as a sub-Keplerian, low angular momentum
flow with shock in the inner region [2]}. Actually they find the global accretion solution that the viscous Keplerian flow with the viscosity parameter \(\alpha \)  (\(\le \)  0.15) at the outer boundary beyond distance of \(5 \times 10^3 r_{\rm g}\)  connects to the low angular momentum sub-Keplerian flow below the inner region of a few hundreds \(r_{\rm g}\) .
